The Remnant and Origin of the Historical Supernova 1181 AD

Ritter, Andreas; Parker, Quentin A.; Lykou, Foteini; Zijlstra, A. A.; Guerrero, M. A.; Dû, Pascal Le

doi:10.3847/2041-8213/ac2253

Cited by 22 publications

(54 citation statements)

References 26 publications

(46 reference statements)

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“…Fernández & Metzger (2013) also bring a detonation ignited in a WD-neutron star merger event into play for SNe Iax. While the historic SN Iax remnant SN 1181 is believed to originate from an ONe-CO WD merger (Oskinova et al 2020;Ritter et al 2021) the SN remnant Sgr A East has recently been associated with a failed deflagration producing a SN Iax (Zhou et al 2021). Hence, the question whether it is possible to explain the entire class of SNe Iax in the framework of the pure deflagration in a M Ch WD model remains.…”

Section: Introductionmentioning

confidence: 99%

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

Lach

Callan

Bubeck

et al. 2022

A&A

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Context. Due to the ever increasing number of observations during the past decades, Type Ia supernovae are nowadays regarded as a heterogeneous class of optical transients consisting of several subtypes. One of the largest of these subclasses is the class of Type Iax supernovae. They have been suggested to originate from pure deflagrations in carbon-oxygen Chandrasekhar mass white dwarfs because the outcome of this explosion scenario is in general agreement with their subluminous nature. Aims. Although a few deflagration studies have already been carried out, the full diversity of the class has not been captured yet. This, in particular, holds for the faint end of the subclass. We therefore present a parameter study of single-spot ignited deflagrations in Chandrasekhar mass white dwarfs varying the location of the ignition spark, the central density, the metallicity, and the composition of the white dwarf. We also explore a rigidly rotating progenitor to investigate whether the effect of rotation can spawn additional trends. Methods. We carried out three-dimensional hydrodynamic simulations employing the LEAFS code. Subsequently, detailed nucleosynthesis results were obtained with the nuclear network code YANN. In order to compare our results to observations, we calculated synthetic spectra and light curves with the ARTIS code. Results. The new set of models extends the range in brightness covered by previous studies to the lower end. Our single-spot ignited explosions produce 56Ni masses from 5.8 × 10−3 to 9.2 × 10−2 M⊙. In spite of the wide exploration of the parameter space, the main characteristics of the models are primarily driven by the mass of 56Ni and form a one-dimensional sequence. Secondary parameters seem to have too little impact to explain the observed trend in the faint part of the Type Iax supernova class. We report kick velocities of the gravitationally bound explosion remnants from 6.9 to 369.8 km s−1. The magnitude as well as the direction of the natal kick is found to depend on the strength of the deflagration. Conclusions. This work corroborates the results of previous studies of deflagrations in Chandrasekhar mass white dwarfs. The wide exploration of the parameter space in initial conditions and viewing angle effects in the radiative transfer lead to a significant spread in the synthetic observables. The trends in observational properties toward the faint end of the class are, however, not reproduced. This motivates a quantification of the systematic uncertainties in the modeling procedure and the influence of the 56Ni-rich bound remnant to get to the bottom of these discrepancies. Moreover, while the pure deflagration scenario remains a favorable explanation for bright and intermediate luminosity Type Iax supernovae, our results suggest that other mechanisms also contribute to this class of events.

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Section: Introductionmentioning

confidence: 99%

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

Lach

Callan

Bubeck

et al. 2022

A&A

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“…The nebula appears circular, approximately 3 -4 across depending on the wavelength of the imagery. Faint, diffuse [O iii] nebular emission is seen via deep narrow-band imaging (Kronberger et al 2014;Oskinova et al 2020;Ritter et al 2021). An [S ii] shell is expanding at 1000 ± 100 km s −1 Paper I.…”

Section: Introductionmentioning

confidence: 99%

A new study on a type Iax stellar remnant and its probable association with SN 1181

Lykou¹,

Parker²,

Ritter³

et al. 2022

Preprint

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We report observations and modelling of the stellar remnant and presumed double-degenerate merger of Type Iax supernova SN 1181 AD. It is the only known bound stellar SN remnant and the only star with Wolf-Rayet features that is neither a planetary nebula central star nor a massive Pop I progenitor. We model the unique emission-line spectrum with broad, strong O vi and O viii lines as a fast stellar wind and shocked, hot gas. Non-LTE wind modeling indicates a mass-loss rate of ∼ 10 −6 M yr −1 and a terminal velocity of ∼15,000 km s −1 , consistent with earlier results. O viii lines indicate shocked gas temperatures of T 4 MK. We derive a magnetic field upper limit of B < 2.5 MG, below earlier suggestions. The luminosity indicates a remnant mass of 1.2 ± 0.2 M with ejecta mass 0.15 ± 0.05 M . Archival photometry suggests the stellar remnant has dimmed by ∼0.5 magnitudes over 100 years. A low Ne/O < 0.15 argues against a O-Ne white dwarf in the merger. A cold dust shell is only the second detection of dust in a SN Iax and the first of cold dust. Our ejecta mass and kinetic energy estimates of the remnant are consistent with Type Iax extragalactic sources.

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“…Fernández & Metzger (2013) also bring a detonation ignited in a WD-neutron star merger event into play for SNe Iax. While the historic SN Iax remnant SN 1181 is believed to originate from an ONe-CO WD merger (Oskinova et al 2020;Ritter et al 2021) the SN remnant Sgr A East has recently been associated with a failed deflagration producing a SN Iax (Zhou et al 2021). Hence, the question remains: is it possible to explain the entire class of SNe Iax in the framework of the pure deflagration in a M Ch WD model?…”

Section: Introductionmentioning

confidence: 99%

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

Lach,

Callan,

Bubeck

et al. 2021

Preprint

View full text Add to dashboard Cite

Context. Due to the ever increasing number of observations during the past decades Type Ia supernovae are nowadays regarded as a heterogeneous class of optical transients consisting of several sub-types. One of the largest of these subclasses is the class of Type Iax supernovae. They have been suggested to originate from pure deflagrations in carbon-oxygen Chandrasekhar-mass white dwarfs because the outcome of this explosion scenario is in general agreement with their sub-luminous nature. Aims. Although a few deflagration studies have already been carried out, the full diversity of the class is not captured yet. This, in particular, holds for the faint end of the subclass. We therefore present a parameter study of single-spot ignited deflagrations in Chandrasekhar-mass white dwarfs varying the location of the ignition spark, the central density, the metallicity and the composition of the white dwarf. We also explore a rigidly rotating progenitor to investigate whether the effect of rotation can spawn additional trends. Methods. We carry out three dimensional hydrodynamic simulations employing the leafs code. Subsequently, detailed nucleosynthesis results are obtained with the nuclear network code yann. In order to compare our results to observations we calculate synthetic spectra and light curves with the artis code. Results. The new set of models extends the range in brightness covered by previous studies to the lower end. Our single-spot ignited explosions produce 56 Ni masses from 5.8 × 10 −3 to 9.2 × 10 −2 M . In spite of the wide exploration of the parameter space the main characteristics of the models are primarily driven by the mass of 56 Ni and form a one-dimensional sequence. Secondary parameters seem to have too little impact to explain the observed trend in the faint part of the Type Iax supernova class. We report kick velocities of the gravitationally bound explosion remnants from 6.9 to 369.8 km s −1 . The magnitude as well as the direction of the natal kick is found to depend on the strength of the deflagration. Conclusions. This work corroborates the results of previous studies of deflagrations in Chandrasekhar-mass white dwarfs. The wide exploration of the parameter space in initial conditions and viewing-angle effects in the radiative transfer lead to a significant spread in the synthetic observables. The trends in observational properties towards the faint end of the class are, however, not reproduced. This motivates a quantification of the systematic uncertainties in the modelling procedure and the influence of the 56 Ni -rich bound remnant to get to the bottom of these discrepancies. Moreover, while the pure deflagration scenario remains a favorable explanation for bright and intermediate luminosity Type Iax supernovae, the possibility that this subclass does not consist of only one explosion scenario needs to be taken into account.

show abstract

The Remnant and Origin of the Historical Supernova 1181 AD

Cited by 22 publications

References 26 publications

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

A new study on a type Iax stellar remnant and its probable association with SN 1181

Type Iax supernovae from deflagrations in Chandrasekhar mass white dwarfs

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